2004A&A...413..895D


Query : 2004A&A...413..895D

2004A&A...413..895D - Astronomy and Astrophysics, volume 413, 895-902 (2004/1-3)

Close and distant reprocessing media in Mkn 509 studied with BeppoSAX.

DE ROSA A., PIRO L., MATT G. and PEROLA G.C.

Abstract (from CDS):

We present the broad band analysis of two BeppoSAX observations of the Seyfert 1 Mkn 509. In 2000 the source was in a typical flux state, F2–10keV=2.7x10–11erg/cm2/s, while in 1998 it was found in a high flux state, F2–10keV=5.7x10–11erg/cm2/s. A comparison between the two states shows a energy-dependent flux variation of about a factor of three and a factor of two in the LECS (0.15-3keV) and MECS (1.5-10keV), respectively, while in the PDS (13-200keV) the difference is marginal. A soft excess, a narrow iron line and a Compton reflection hump above 10keV are clearly apparent in the residuals after fitting the spectra with a simple power law. We tested two alternative models. In the first the iron line and the high energy bump are well reproduced by reprocessing in a cold and Compton thick material. The intensity of the iron line (also consistent with a Chandra measurement) as well as the normalization of the reflection hump are consistent with a constant in the two epochs: this, combined with the fact that the line is narrow as observed by Chandra, suggests a common origin from distant and optically thick matter. This model further requires a component to model the soft excess: the empirical choice of two black bodies accounts well for the excess in both observations; their combined strength was a factor of about three higher in the high than in the low flux state defined above. However, the relative contribution of the soft excess is higher in the low flux state. In the second model we attempted to reproduce all spectral features, except for the narrow cold line, with reflection from an ionized disc. This model is successful only in the high flux state, but it fails in the low flux state, when the soft excess is only partially accounted for. In either model, the slope of the power law is greater in the high than in the low flux state, (ΔΓ∼0.2), in agreement with a behaviour known to be shared by several objects of the same type.

Abstract Copyright:

Journal keyword(s): galaxies: individual: Mkn 509 - galaxies: Seyfert - X-rays: galaxies

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 LB 1727 Sy1 04 26 00.7188165240 -57 12 01.769902992 13.68 14.58 14.37 14.8   ~ 252 0
2 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1553 0
3 NGC 4151 Sy1 12 10 32.5759813872 +39 24 21.063527532   12.18 11.48     ~ 3525 2
4 Mrk 205 Sy1 12 21 44.0724099888 +75 18 38.241006228   15.64 15.24 14.7   ~ 458 0
5 IC 4271 Sy2 13 29 21.4493074392 +37 24 50.460172056   15.6       ~ 123 1
6 ESO 445-50 Sy1 13 49 19.2601801224 -30 18 34.213815504   13.81 13.66 12.18   ~ 759 0
7 NGC 5506 AGN 14 13 14.8761010056 -03 12 27.556909272   15.25 14.38     ~ 1046 0
8 NGC 5548 Sy1 14 17 59.5400291832 +25 08 12.603122268   14.35 13.73     ~ 2536 0
9 Mrk 509 Sy1 20 44 09.7504483224 -10 43 24.727155528   13.35 13.12 10.7   ~ 1199 0
10 NGC 7213 Sy1 22 09 16.2100443720 -47 10 00.115999716   10.97 12.08 10.50 10.6 ~ 620 0
11 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1994 3

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2022.06.28-17:36:35

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